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Antares Collaboration

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Presentation on theme: "Antares Collaboration"— Presentation transcript:

1 Antares Collaboration
Eleonora Presani Antares Collaboration – Nikhef – Amsterdam

2 Concept of Neutrino detector
Natural radiator is low cost and allows huge instrumented regions Has very little light scattering. blue light produced by charged particles with v>c/n optical sensors detect the time and charge produced by light 16 January 2019 Eleonora Presani - NOW2008

3 The ANTARES neutrino telescope
60 m 500 m 15 m -2475 m 40 km 900 PMTs 12 lines 25 storeys/line 3 PMTs/storey 16 January 2019 Eleonora Presani - NOW2008

4 Status until 2006 16 January 2019 Eleonora Presani - NOW2008
June 1889: L’Institut Michel Pacha Status until 2006 (40 km) Oct. ’01: MEO Cable Dec. ’02: Junction Box Dec. ’06: Line 3 Mar. ’06: Line 1 Mar. ’05: MILOM Sept. ’06: Line 2 16 January 2019 Eleonora Presani - NOW2008

5 Status during 2007 16 January 2019 Eleonora Presani - NOW2008 Jan ’07:
Lines 4 & 5, Line connection Mar. ’07: Line 6 Apr. ’07: Line 7 Apr./July ’07: MILOM -> IL07 July ’07: Lines 8 & 9 Nov. ’07: Line 10 Dec. ’07: Line connection 16 January 2019 Eleonora Presani - NOW2008

6 Detector Completed! 16 January 2019 Eleonora Presani - NOW2008
March-May 2008: Lines 11 & 12, connection 2008 – 2xxx: Lots of physics data! 16 January 2019 Eleonora Presani - NOW2008

7 Other available triggers:
Software Trigger Full sky trigger: All data sent to shore through Gb links and filtered looking for directions for light signals compatible with a muon track Other available triggers: 1D Trigger following the Galactic Center GRB Trigger with GRB stellite alert Monopole trigger ... Trigger rate: ̃2-3 Hz (10 Lines) All muons!!! 16 January 2019 Eleonora Presani - NOW2008

8 Background light rate Median counting rate in 10” PMT in Line 1
Proportion of time < rate Median counting rate in 10” PMT in Line 1 March 2006 – May 2008 16 January 2019 Eleonora Presani - NOW2008

9 Effective area & angular resolution
ANTARES 12 lines 16 January 2019 Eleonora Presani - NOW2008

10 Time resolution RMS <1 ns On shore laser system RMS <1 ns In sea
Optical fibres Laser RMS <1 ns In sea LED beacon system LED beacon 16 January 2019 Eleonora Presani - NOW2008

11 Reconstruction of a muon track
Reconstruction with Line1: Algorithm minimizes χ2 of PMT hit time vs. altitude to find zenith angle of m track Online Data filter : Look for local coincidences (trigger hits) within 20ns Ask for ≥ 5 trigger hits Antares preliminary Hit time [ns] Hit altitude (relative to mid detector) [m] Triggered hits Hits used in fit Snapshot hits + Run 21240 Event 13212 Zenith θ = 147o μ 16 January 2019 Eleonora Presani - NOW2008

12 Data taking with the 12lines detector
Detector footprint from atmospheric muons Bright muon bundle event ! Neutrino candidate 16 January 2019 Eleonora Presani - NOW2008 12

13 Event Display 16 January 2019 Eleonora Presani - NOW2008

14 Methods for the search of point-like sources
Different methods has been developed within ANTARES collaboration for the search for point-like sources: Grid/Cluster ML Ratio EM algorithm Unbinned techniques Binned techniques Signal-like Background-like Signal-like Background-like 16 January 2019 Eleonora Presani - NOW2008

15 Expected Limits for point sources
ANTARES 1 yr 16 January 2019 Eleonora Presani - NOW2008

16 Neutrinos? neutrinos! rate [Hz] q d(q ) Earth muon cos q

17 cosmic micro-wave background
What to do with them? Dark Matter Monopoles 15 billion years Life χ Today T = 2.7 K - ν νμ γc θc = 42º Galaxy formation Solar system decoupling of cosmic micro-wave background 400,000 years Matter recombination T = 3000 K Indirect detection of WIMPs using neutrino telescopes: Relic WIMPs from the Big Bang traversing the universe undergo multiple elastic interactions with inside a massive celestial object (e.g. the Sun), lose kinetic energy and become gravitationally bound to the object. Over time, the WIMP density in the core of the object increases. This enhances the WIMP annihilation rate significantly, resulting in a neutrino flux with energies up to 400 GeV that will reach the Earth. These neutrinos can interact through a CC interaction in the vicinity of a neutrino telescope, producing an energetic muon. When traversing the transparent medium of the telescope, the muon will emit Cherenkov light. By measuring the time & position of the photons using a 3D grid of PMTs, the neutrino track can be reconstructed. 1 s History of Universe light elements Nucleosynthesis 1 MeV 10-6 s protons, neutrons quark-hadron transition 1 GeV 10-11 s Separation of EM and weak forces Electro-weak phase transition 103 GeV Super-symmetry? 10-35 s Baryogenesis Grand Unification transition 1015 GeV 10-43 s Quantum gravity barrier Big Bang 16 January 2019 Eleonora Presani - NOW2008 1019 GeV

18 before, during and after
Gamma-Ray Burst What to do with them? Tau Neutrino Name Baloon Lollipop Inverted Lollipop Sugardaddy (T. DeYoung - IceCube) Double Bang Gamma Ray Bursts Tau Neutrinos nt t All data nt t detector alert x 2–10 nt t m location of GRB Volume save nt t All data before, during and after GRB analysis 16 January 2019 Eleonora Presani - NOW2008

19 Questions??? Conclusions ANTARES is completed!
First data are being analyzed and neutrinos are extracted from atmospheric muon background Calibrations ensure an angular resolution at the level of 0.2 degrees > 10 TeV of neutrino energy The systematic errors are already under study Astronomy is a reality in ANTARES!! Questions??? 16 January 2019 Eleonora Presani - NOW2008

20 Backup slides 16 January 2019 Eleonora Presani - NOW2008

21 Cable Fix 16 January 2019 Eleonora Presani - NOW2008

22 Outlook The ANTARES collaboration Detector COMPLETED!
Performances of Antares Calibration Trigger and reconstruction First results! Expected limits Conclusions 16 January 2019 Eleonora Presani - NOW2008

23 Amplitude Calibration
Example 1: Threshold value in photo electron equivalent units Example 2: Counting rate on single photomultiplier Before calibration After calibration 16 January 2019 Eleonora Presani - NOW2008

24 Detector understanding
Water absorption length ±10% variation OM angular acceptance Different parameterisations 16 January 2019 Eleonora Presani - NOW2008

25 Project history 1996 - 2000 Measurements with autonomous lines
3) Optical properties study: deployments Optical background study: deployments 2) Biofouling-sedimentation study: deployments 45 km long EOC developed in 2001 The Junction box, the heart of the array for data and HV distribution, installed in Dec 2002 works perfectly 16 January 2019 Eleonora Presani - NOW2008

26 The angular distribution
Data Atmospheric Neutrino Monte Carlo Atmospheric Muon Monte Carlo Multi line fit Single line fit 78 neutrinos 36 neutrinos 16 January 2019 Eleonora Presani - NOW2008

27 GRB Trigger In some cases, data are recorded even before the alert
Out of 198 GCN triggers 176 have been handled by Antares DAQ 16 January 2019 Eleonora Presani - NOW2008 M. Spurio- ANTARES 27

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